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Title: Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions

Abstract

The transport of cosmic rays (CRs) in the heliosphere is determined by the properties of the solar wind plasma. The heliospheric plasma environment has been probed by spacecraft for decades and provides a unique opportunity for testing transport theories. Of particular interest for the three-dimensional (3D) heliospheric CR transport are structures such as corotating interaction regions (CIRs), which, due to the enhancement of the magnetic field strength and magnetic fluctuations within and due to the associated shocks as well as stream interfaces, do influence the CR diffusion and drift. In a three-fold series of papers, we investigate these effects by modeling inner-heliospheric solar wind conditions with the numerical magnetohydrodynamic (MHD) framework Cronos (Wiengarten et al., referred as Paper I), and the results serve as input to a transport code employing a stochastic differential equation approach (this paper). While, in Paper I, we presented results from 3D simulations with Cronos, the MHD output is now taken as an input to the CR transport modeling. We discuss the diffusion and drift behavior of Galactic cosmic rays using the example of different theories, and study the effects of CIRs on these transport processes. In particular, we point out the wide range of possiblemore » particle fluxes at a given point in space resulting from these different theories. The restriction of this variety by fitting the numerical results to spacecraft data will be the subject of the third paper of this series.« less

Authors:
 [1]; ;  [2];  [3]; ;  [4]; ;  [5]
  1. Université Libre de Bruxelles, Service de Physique Statistique et des Plasmas, CP 231, B-1050 Brussels (Belgium)
  2. Institut für Theoretische Physik IV, Ruhr-Universität Bochum, D-44780 Bochum (Germany)
  3. Department of Physics and KIPAC, Stanford University, Stanford, CA 94305 (United States)
  4. Institut für Experimentelle und Angewandte Physik, Christian-Albrecht-Universität zu Kiel, D-24098 Kiel (Germany)
  5. Centre for Space Research, North-West University, 2520 Potchefstroom (South Africa)
Publication Date:
OSTI Identifier:
22661328
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal; Journal Volume: 837; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COSMIC RADIATION; DIFFERENTIAL EQUATIONS; DIFFUSION; HELIOSPHERE; INTERACTIONS; INTERFACES; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; PLASMA; SIMULATION; SOLAR WIND; SPACE; SPACE VEHICLES; STOCHASTIC PROCESSES; STREAMS; SUN; THREE-DIMENSIONAL CALCULATIONS; TRANSPORT THEORY

Citation Formats

Kopp, Andreas, Wiengarten, Tobias, Fichtner, Horst, Effenberger, Frederic, Kühl, Patrick, Heber, Bernd, Raath, Jan-Louis, and Potgieter, Marius S. Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions. United States: N. p., 2017. Web. doi:10.3847/1538-4357/AA603B.
Kopp, Andreas, Wiengarten, Tobias, Fichtner, Horst, Effenberger, Frederic, Kühl, Patrick, Heber, Bernd, Raath, Jan-Louis, & Potgieter, Marius S. Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions. United States. doi:10.3847/1538-4357/AA603B.
Kopp, Andreas, Wiengarten, Tobias, Fichtner, Horst, Effenberger, Frederic, Kühl, Patrick, Heber, Bernd, Raath, Jan-Louis, and Potgieter, Marius S. Wed . "Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions". United States. doi:10.3847/1538-4357/AA603B.
@article{osti_22661328,
title = {Cosmic-Ray Transport in Heliospheric Magnetic Structures. II. Modeling Particle Transport through Corotating Interaction Regions},
author = {Kopp, Andreas and Wiengarten, Tobias and Fichtner, Horst and Effenberger, Frederic and Kühl, Patrick and Heber, Bernd and Raath, Jan-Louis and Potgieter, Marius S.},
abstractNote = {The transport of cosmic rays (CRs) in the heliosphere is determined by the properties of the solar wind plasma. The heliospheric plasma environment has been probed by spacecraft for decades and provides a unique opportunity for testing transport theories. Of particular interest for the three-dimensional (3D) heliospheric CR transport are structures such as corotating interaction regions (CIRs), which, due to the enhancement of the magnetic field strength and magnetic fluctuations within and due to the associated shocks as well as stream interfaces, do influence the CR diffusion and drift. In a three-fold series of papers, we investigate these effects by modeling inner-heliospheric solar wind conditions with the numerical magnetohydrodynamic (MHD) framework Cronos (Wiengarten et al., referred as Paper I), and the results serve as input to a transport code employing a stochastic differential equation approach (this paper). While, in Paper I, we presented results from 3D simulations with Cronos, the MHD output is now taken as an input to the CR transport modeling. We discuss the diffusion and drift behavior of Galactic cosmic rays using the example of different theories, and study the effects of CIRs on these transport processes. In particular, we point out the wide range of possible particle fluxes at a given point in space resulting from these different theories. The restriction of this variety by fitting the numerical results to spacecraft data will be the subject of the third paper of this series.},
doi = {10.3847/1538-4357/AA603B},
journal = {Astrophysical Journal},
number = 1,
volume = 837,
place = {United States},
year = {Wed Mar 01 00:00:00 EST 2017},
month = {Wed Mar 01 00:00:00 EST 2017}
}